LIGO-G050484-00-R LIGO R&D1 Improvement of the MGAS Filter Damping Performance Alberto Stochino University of Pisa, Italy SURF Student Mentor: Dr. Riccardo.

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Presentation transcript:

LIGO-G R LIGO R&D1 Improvement of the MGAS Filter Damping Performance Alberto Stochino University of Pisa, Italy SURF Student Mentor: Dr. Riccardo De Salvo

LIGO-G R LIGO R&D2 Seismic Noise Noise Budget It is the disturbance resulting from the displacement of the mirrors due to the ground motion seismic

LIGO-G R LIGO R&D3 The vertical and horizontal degrees of freedom are not independent mechanical complexity non uniformity of the terrestrial gravitational field Vertical Motion of the Mirrors the motion of the mirrors in the vertical direction can change the arm length of the interferometer

LIGO-G R LIGO R&D4 Vertical Attenuation ground motion ~ m expected GW signal ~ m required attenuation factor ~ vertical to horizontal couplings must not be limiting factors to the horizontal sensibility ~< 10e-3 Gravitational Coupling negligible respect to other couplings ~ 1%

LIGO-G R LIGO R&D5 Passive Mechanical Filters Massive spring

LIGO-G R LIGO R&D6 The C.O.P. Effect limitation on attenuation performance Center Of Percussion

LIGO-G R LIGO R&D7 MGAS Filter Linear Model for GAS Springs

LIGO-G R LIGO R&D8 GAS Filter Limit (Kenji Numata) Transfer Function COP limit

LIGO-G R LIGO R&D9 Inverted Pendulum Transfer Function

LIGO-G R LIGO R&D10 C.O.P. Displacement Transfer Function for the counterweighted IP

LIGO-G R LIGO R&D11 Extending the Idea to the GAS Springs M noise cop What we had before What we wanted to do blade

LIGO-G R LIGO R&D12 Prototype Design

LIGO-G R LIGO R&D13 Making it Real

LIGO-G R LIGO R&D14 Tuning of the Counterweight

LIGO-G R LIGO R&D15 Experiment Setup 1) GAS blade 2) Filter body 3) Support spring 4) Voice-coil 5) Payload 6) Rigid connector 7) Accelerometer

LIGO-G R LIGO R&D16 The Initial TF

LIGO-G R LIGO R&D17 Overcompensation Three Booms No CWs

LIGO-G R LIGO R&D18 Three Booms + 2x3 CWs Note the phase advance

LIGO-G R LIGO R&D19 Undercompensation Two Booms No CWs

LIGO-G R LIGO R&D20 Two Booms + 1 CW

LIGO-G R LIGO R&D21 Two Booms + ½ CW ?

LIGO-G R LIGO R&D22 Two Booms 1 CW CW positions comparison

LIGO-G R LIGO R&D23 Two Booms 1 CW Inner

LIGO-G R LIGO R&D24 E.M. Antispring Circuitry

LIGO-G R LIGO R&D25 E.M. Antispring Two Booms 1 CW Inner

LIGO-G R LIGO R&D26 Next Lower the noise at high frequencies Deepen the TF and Phase data analysis Find the optimal setup for the best compensation HAM-SAS

LIGO-G R LIGO R&D27 Acknowledgments Dr. Riccardo DeSalvo Virginio Sannibale Francesco Fidecaro The LIGO-SURF Program The NSF Caltech Pasadena, California, USA

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